HUBBLE SPACE TELESCOPE
DAILY REPORT # 3127
PERIOD COVERED: 0000Z (UTC) 05/29/02 - 0000Z (UTC) 05/30/02
OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
NICMOS 8790
NICMOS Post-SAA calibration - CR Persistence Part 1.
A new procedure proposed to alleviate the CR-persistence problem of NICMOS.
Dark
frames will be obtained immediately upon exiting the SAA contour 23, and every
time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.
The darks will be obtained in parallel in all three NICMOS Cameras. The
POST-SAA
darks will be non-standard reference files available to users with a USEAFTER
date/time mark.
STIS/CCD 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.
STIS/CCD 8904
Bias Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in
the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order
to build up high-S/N superbiases and track the evolution of hot columns.
WFPC2 8938
WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.
characterizing the evolution of hot pixels.
WF/PC-2 8941
Cycle 10 UV Earthflats.
improve the quality of pipeline flat fields for the WFPC2 UV filter set.
ACS/WFC/HRC 8947
Weekly Test.
The Advanced Camera for Surveys (WFC and HRC) was used to perform basic
tests to
monitor, the read noise, the development of hot pixels and test for any source
of noise in ACS CCD detectors. This program will be executed at least once
a day
for the entire lifetime of ACS.
ACS/HRC 9012
HRC Coronagraph Acquisition.
The Advanced Camera for Surveys (HRC) was used to verify the abilities of the
flight and ground software to perform isolated point-source acquisition
onto the
coronagraph occulting spots and the Fastie Finger. Successful execution of
these
acquisitions will also demonstrate the ability of the software to calculate the
centroid of the target positions and to perform automated telescope pointing.
ACS 9023
ACS SBC Image Quality Verification
This activity will obtain a series of images to evaluate the point source image
quality over the field of view of the ACS SBC channel, after the corrector
mechanisms have been used to optimize the image focus and symmetry using
the HRC
channel. NGC 6681 {18.7 h, -32 deg} will be the target, as this star field has
been used extensively by the STIS program for UV PSF measurement and
photometry.
High SNR images will be obtained in the F125LP and F150LP filters, with dithers
in each axis. Images will also be obtained with the F122M filter, at lower SNR,
for direct comparison with CEI specs at Lyman alpha. The field will also be
observed with the HRC {F250W} to establish the relative aperture
location/orientation.
STIS/CCD 9066
Closing in on the Hydrogen Reionization Edge of the Universe.
The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain
the Hydrogen reionization edge in emission that marks the transition from a
neutral to a fully ionized IGM at a predicted redshifts.
ACS/WFC/HRC 9075
Cosmological Parameters from Type Ia Supernovae at High Redshift.
{SNe Ia} that will be of long lasting value as a record of the expansion
history
of the universe.
NICMOS 9269
NICMOS Parallel Thermal Background
NICMOS Camera 3 pure parallel exposures in the F222M filter will be
obtained for
the entire duration of SMOV to establish the stability of the
HST+NCS+Instrument
thermal emission.
STIS/CCD 9317
Pure Parallel Imaging Program: Cycle 10.
The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.
WF/PC-2 9318
POMS Test Proposal: WFII Parallel Archive Proposal Continuation.
The WF/PC-2 was used to perform the generic target version of the WFPC2
Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working
Group.
NICMOS 9326
NICMOS Cycle 10 Early Calibration Monitor
This calibration program is the early Cycle 10 NICMOS monthly monitor
program. A
series of flat field observations will be obtain to monitor the stability and
health of the NICMOS detectors.
STIS/FUV 9412
The Physical Parameters of the Hottest, Most Luminous Stars as a Function of
Metallicity
We have obtained excellent, new ground-based blue optical and HAlpha spectra of
a sample of very early-type stars in the Magellanic Clouds in order to measure
their physical properties, for comparison with the extensive data that exists
for higher-metallicity Galactic stars. Our aim is to understand how effective
temperatures depend upon metallicity {necessary in determining IMFs}, and to
explore the astrophysically interesting regime of stars of extreme
temperatures,
masses, and luminosities. In order to do this, we need to measure the stellar
wind terminal velocities for our stars, necessary to constrain the stellar
models. These can only be measured with STIS/FUV on HST. In addition, we will
obtain higher spatial resolution data on the HAlpha line for stars for which
nebular contamination is significant in our ground-based data. We also include
several R136 stars with excellent STIS/CCD data but which lack UV line
measures.
These new HST data will provide important information about the strengths of
stellar winds at extreme luminosities and the calibration of the Wind Momentum-
Luminosity Relationship at lower metallicities. This proposal was highly rated
in Cycle 9, but only 4 snapshots were obtained. We have completed the analysis
of these plus additional data from the archives, but need spectra of the
remaining objects if we are to answer the questions we pose.
ACS/WFC 9575
Default {Archival} Pure Parallel Program.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.
FLIGHT OPERATIONS SUMMARY:
HSTARs:
8666 Fep Q channel DMT FOF queue buffer overflow" C-string @ 149/12:41z
8667 GSacq (3,2,3) results in Fine Lock Backup (3,0,3) @ 151/06:29:30z
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 9 9
FGS REacq 10 10
FHST Update 21 21
LOSS of LOCK None
Operations Notes:
FOT is now in building 23 with C String Prime, Due to isolation test.
SIGNIFICANT EVENTS:
Continuation of Servicing Mission Orbital Verification and the gradual
resumption of normal science observations and calibrations.